Onset mechanism of an inverted U-shaped solar filament eruption revealed by NVST, SDO, and STEREO-A observations

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Fig. 11.

Distribution of the magnetic pressure in the white box of Fig. 9a. (a)–(b): magnetic pressure at 05:48 UT and 07:12 UT. The contours outline the magnetic pressure with levels of 1000, 2000, 5000, and 10 000 dyn/cm². (c) Variation in the mean gradient of the magnetic pressure in the black box of panel a.

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